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Title: Outflow Kinematics Manifested by the Hα Line: Gas Outflows in Type 2 AGNs. IV

Abstract

Energetic ionized gas outflows driven by active galactic nuclei (AGNs) have been studied as a key phenomenon related to AGN feedback. To probe the kinematics of the gas in the narrow-line region, [O iii] λ 5007 has been utilized in a number of studies showing nonvirial kinematic properties due to AGN outflows. In this paper, we statistically investigate whether the H α emission line is influenced by AGN-driven outflows by measuring the kinematic properties based on the H α line profile and comparing them with those of [O iii]. Using the spatially integrated spectra of ∼37,000 Type 2 AGNs at z < 0.3 selected from the Sloan Digital Sky Survey DR7, we find a nonlinear correlation between H α velocity dispersion and stellar velocity dispersion that reveals the presence of the nongravitational component, especially for AGNs with a wing component in H α . The large H α velocity dispersion and velocity shift of luminous AGNs are clear evidence of AGN outflow impacts on hydrogen gas, while relatively smaller kinematic properties compared to those of [O iii] imply that the observed outflow effect on the H α line is weaker than the case of [O iii].

Authors:
; ;  [1]
  1. Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 151-742 (Korea, Republic of)
Publication Date:
OSTI Identifier:
22663223
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 845; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BALMER LINES; COMPARATIVE EVALUATIONS; CORRELATIONS; DISPERSIONS; EMISSION; FEEDBACK; GALAXIES; GALAXY NUCLEI; HYDROGEN; QUASARS; SPECTRA; VELOCITY

Citation Formats

Kang, Daeun, Woo, Jong-Hak, and Bae, Hyun-Jin, E-mail: woo@astro.snu.ac.kr. Outflow Kinematics Manifested by the Hα Line: Gas Outflows in Type 2 AGNs. IV. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA80E8.
Kang, Daeun, Woo, Jong-Hak, & Bae, Hyun-Jin, E-mail: woo@astro.snu.ac.kr. Outflow Kinematics Manifested by the Hα Line: Gas Outflows in Type 2 AGNs. IV. United States. doi:10.3847/1538-4357/AA80E8.
Kang, Daeun, Woo, Jong-Hak, and Bae, Hyun-Jin, E-mail: woo@astro.snu.ac.kr. Sun . "Outflow Kinematics Manifested by the Hα Line: Gas Outflows in Type 2 AGNs. IV". United States. doi:10.3847/1538-4357/AA80E8.
@article{osti_22663223,
title = {Outflow Kinematics Manifested by the Hα Line: Gas Outflows in Type 2 AGNs. IV},
author = {Kang, Daeun and Woo, Jong-Hak and Bae, Hyun-Jin, E-mail: woo@astro.snu.ac.kr},
abstractNote = {Energetic ionized gas outflows driven by active galactic nuclei (AGNs) have been studied as a key phenomenon related to AGN feedback. To probe the kinematics of the gas in the narrow-line region, [O iii] λ 5007 has been utilized in a number of studies showing nonvirial kinematic properties due to AGN outflows. In this paper, we statistically investigate whether the H α emission line is influenced by AGN-driven outflows by measuring the kinematic properties based on the H α line profile and comparing them with those of [O iii]. Using the spatially integrated spectra of ∼37,000 Type 2 AGNs at z < 0.3 selected from the Sloan Digital Sky Survey DR7, we find a nonlinear correlation between H α velocity dispersion and stellar velocity dispersion that reveals the presence of the nongravitational component, especially for AGNs with a wing component in H α . The large H α velocity dispersion and velocity shift of luminous AGNs are clear evidence of AGN outflow impacts on hydrogen gas, while relatively smaller kinematic properties compared to those of [O iii] imply that the observed outflow effect on the H α line is weaker than the case of [O iii].},
doi = {10.3847/1538-4357/AA80E8},
journal = {Astrophysical Journal},
number = 2,
volume = 845,
place = {United States},
year = {Sun Aug 20 00:00:00 EDT 2017},
month = {Sun Aug 20 00:00:00 EDT 2017}
}